南京大学学报(自然科学版) ›› 2021, Vol. 57 ›› Issue (6): 981–999.doi: 10.13232/j.cnki.jnju.2021.06.007

• • 上一篇    下一篇

水星的火山活动历史

王一尘1, 肖智勇1,2()   

  1. 1.行星环境与宜居性研究实验室，中山大学大气科学学院，珠海，519082
    2.中国科学院比较行星学卓越创新中心，合肥，230026
  • 收稿日期:2021-08-25 出版日期:2021-11-30 发布日期:2021-12-03
  • 通讯作者: 肖智勇 E-mail:xiaozhiyong@mail.sysu.edu.cn
  • 作者简介:E⁃mail：xiaozhiyong@mail.sysu.edu.cn
  • 基金资助:
    国家自然科学基金(41773063);中国科学院前沿重点部署项目(QYZDY?SSW?DQC028)

The history of volcanism on Mercury

Yichen Wang1, Zhiyong Xiao1,2()   

  1. 1.Planetary Environmental and Astrobiological Research Laboratory，School of Atmospheric Sciences，Sun Yat?sen University，Zhuhai，519082，China
    2.CAS Center for Excellence in Comparative Planetary，Hefei，230026，China
  • Received:2021-08-25 Online:2021-11-30 Published:2021-12-03
  • Contact: Zhiyong Xiao E-mail:xiaozhiyong@mail.sysu.edu.cn

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摘要：

火山活动是天体内部热活动的表现，火山活动的形式和持续时间是探索行星环境和宜居性演化的重要方面.与内太阳系的其他天体一样，水星表面经历了大规模和长时期的火山活动，但是水星上的火山地貌、喷发机制、持续时间，以及火成岩的物质组成等特点和其他类地天体明显不同.水星上的火山活动主要发生在太阳系形成之初的10亿年内，溢流性火山活动形成的坑间平原和平坦平原在全球分布，是水星表面分布面积最大的火山物质.随着内部逐渐冷却，水星自约38亿年前后进入了全球收缩的热状态，岩石圈内的压应力阻碍岩浆上涌，大规模溢流性火山活动快速停止.距今约35亿年以来，水星表面的火山活动主要是挥发分驱动岩浆沿岩石圈内的薄弱带快速上升引起的爆发性火山活动，在全球形成了百余处火成碎屑沉积物.一些爆发性火山活动持续到水星地质历史的近期.水星火山活动的历史反映了独特的幔部动力过程，揭示了天体撞击作用对内部热扰动的影响，对水星的起源和演化具有重要的指示意义.

关键词: 水星, 火山活动, 信使号, 热演化, 熔岩平原, 爆发性火山活动

Abstract:

Volcanism is the manifestation of internal thermal activity，and the style and history of volcanism are important target to resolve the evolution of planetary surface enviroment and habitability. Similar with the other terrestrial bodies，the planet Mercury has been resurfaced by large?scale and long?term volcanic activities. However，characteristics of volcanism on Mercury，such as the compositions，volcanic landforms，eruption mechanisms，and active durations are obviously different from those of the Earth，Mars and Venus. Global effusive volcanism on Mercury occurred within the first billion years of its history and formed intercrater plains and smooth plains that cover a significant portion of the planet. Large?volume effusive volcanism was ceased at about 3.5 Ga due to interior cooling，thus the induced global contraction caused compressive stresses in the lithosphere，impeding the ascent of magma. Afterward，volcanism on Mercury has been shifted to small?scale explosive volcanism that is drived by volatile?rich magma along pre?existing crustal weakness. Explosive volcanism may continue to Mercury'?s recent history. The history of volcanism on Merury reflects special geodynamical process in the mantle，revealing the significant effect of basin?impacts on thermal evolution and providing insights into the origin and evolution of Mercury.

Key words: Mercury, volcanism, MESSENGER, thermal evolution, lava plains, explosive volcanism

中图分类号: 

  • P691

图1

水星表面主要火山地貌（a）水星表面主要火山地貌的空间分布，底图为全球增强彩色镶嵌图，RGB分别对应第二主成分（PC2）、第一主成分（PC1）、430~1000 nm反照率比值；（b，e）水星表面典型平坦平原（中央经纬度59.1°N，38.5°E），内部存在幽灵撞击坑（红色箭头所示）和皱脊（黄色箭头所示）；（c，f）水星表面典型坑间平原（中央经纬度45.4°N，52.5°W）；（d，g）水星表面典型火山口和火成碎屑沉积物（中央经纬度3.2°N，50.1°E）"

表1

水星表面各类地球化学单元的元素分布特征[21]（数据来源于信使号XRS）"

中高钾单元(IHK)

高铝单元

(HAl)

北部平原低镁

单元(N?LMg)

北部平原高镁

单元(N?HMg)

拉赫马尼诺夫

盆地(RB)

高镁单元

(HMg)

低镁高铝单元

(LMg?HAl)

元素丰度比(标准差)，除钾元素外均为质量比，钾元素单位为：1×10-6
Mg/Si0.42 (0.02)0.38 (0.02)0.20 (0.02)0.47 (0.03)0.52 (0.03)0.64 (0.04)0.28 (0.03)
Al/Si0.22 (0.00)0.33 (0.01)0.15 (0.01)0.26 (0.02)0.25 (0.01)0.20 (0.02)0.32 (0.01)
Ca/Si0.16 (0.02)0.16 (0.01)0.15 (0.04)0.15 (0.03)0.16 (0.01)0.23 (0.02)0.15 (0.01)
S/Si0.06 (0.01)0.08 (0.01)0.07 (0.01)0.07 (0.01)0.05 (0.01)0.12 (0.01)0.05 (0.01)
Fe/Si0.06*0.06*0.06 (0.01)0.06*0.06*0.07 (0.01)0.03 (0.01)
Na/Si0.11 (0.02)0.11 (0.02)0.19 (0.04)0.11 (0.02)0.11 (0.02)0.11 (0.02)0.11 (0.02)
K1511 (186)525 (0)1755 (127)1027 (262)1148 (156)1382 (416)803 (266)
基于元素丰度计算所得氧化物含量(标准误差传递)（wt%）
SiO257.2455.0764.0655.0654.1150.8758.88
Al2O311.12 (0.00)16.05 (0.49)8.49 (0.57)12.64 (0.97)11.95 (0.48)8.99 (0.90)16.64 (0.52)
FeO2.07*1.99*2.31 (0.00)1.99*1.95*2.14 (0.00)1.06 (0.00)
MgO18.63 (0.89)16.22 (0.85)9.93 (0.99)20.06 (1.28)21.81 (1.26)25.23 (1.58)12.78 (1.37)
CaO5.99 (0.75)5.76 (0.36)6.28 (1.68)5.40 (1.08)5.66 (0.35)7.65 (0.67)5.78 (0.39)
Na2O3.97 (0.72)3.82 (0.69)7.67 (1.61)3.82 (0.69)3.75 (0.68)3.53 (0.64)4.08 (0.74)
K2O0.18 (0.02)0.06 (0.00)0.21 (0.02)0.12 (0.03)0.14 (0.02)0.17 (0.05)0.10 (0.03)
S1.61 (0.27)2.06 (0.26)2.10 (0.30)1.80 (0.26)1.26 (0.25)2.85 (0.24)1.38 (0.28)
-O=S0.801.031.050.900.631.430.69 (0.14)
总和100.00100.00100.00100.00100.00100.00100.00

IUGS

分类

科马提质安

山岩

玻安质

玄武安山岩

玻安质

粗面岩

科马提质

玄武安山岩

科马提质玄武安山岩科马提质玄武岩玻安质安山岩

图2

水星表面火成岩分类图解[21]（a）水星表面七个地球化学单元的TAS图解，引自Peplowski and Stockstill?Cahill［21］；（b，d）IUGS岩石学分类图解，（c）显示不同地球化学单元间斜长石组分的变化，引自Peplowski and Stockstill?Cahill［21］"

表2

实验岩石学模拟估算的水星表面各地球化学单元的标准矿物组成[21]"

中高钾单元(IHK)高铝单元(HAl)

北部平原低镁单元

(N?LMg)

北部平原高镁单元

(N?HMg)

拉赫马尼诺夫盆地(RB)高镁单元(HMg)

低镁高铝单元

(LMg?HAl)

Qtz--11---5
Or1<11<1<11<1
Plag47 (An26)61 (An45)44 (An0)51 (An34)48 (An33)39 (An34)63 (An44)
Neph-----<1-
Diop14125810241
Hy3032132515-30
Oliv85-152736-
Ns--5----
总和10099999910010099
Tliqa (°C)1464.651410.941304.101485.351518.751533.981336.91
Viscb (Pa?s-1)2.797.5882.01.820.8760.42751.2

图3

水星表面撞击坑N(20)密度[37]N（20）表示每百万平方千米内直径大于20 km的撞击坑密度，计算方法参照文献［37］"

图4

水星上坑间平原的演化过程（a，b）二次撞击坑的累积可以将平坦平原转变为坑间平原［5］，黄色虚线为Denevi et al［6］圈定的平坦平原的边界；（c，d）维尔瓦第区域内坑间平原（白色虚线）与平坦平原（黑色实线），部分20~100 km直径撞击坑挖掘出下伏高反照率平原物质（白色圆圈所示），黑色圆圈标示出挖掘出低反照率物质的相似直径的撞击坑"

图5

全球平坦平原分布[8](a)水星表面不同成因平坦平原的全球分布特征；(b，c)达利撞击坑(45.2°N，119.7°E)内部火山成因的平坦平原；(d，e)杜尔姆斯平原(31.1°S，9.2°E)内疑似火山成因的平坦平原，(e)中白色箭头指示幽灵撞击坑；(f，g)纳博科夫撞击坑(14.6°S，55.7°E)内未知成因的平坦平原"

图6

水星表面的熔岩渠道熔岩渠道首部的火山口（黄色箭头所示）以及熔岩渠道内部的泪滴状残丘（白色箭头所示），长轴方向指示熔岩流动方向"

图7

平坦平原的空间分布与表面地形(a)和壳厚度(b)的对比关系[8]"

图8

水星表面典型火山口和火成碎屑沉积物（a）拉赫马尼诺夫盆地北东侧火成碎屑沉积物，底图为主成分增强彩色镶嵌图；（b）MDIS WAC假彩色图像；（c）基于信使号XRS数据的S/Si分布图［17］；（d）MASCS可见光?近红外相对反照率光谱［30］.HRP：高反照率平原；IP：中间平原；LBP：低反照率蓝色平原；LRM：低反照率物质"

图9

水星表面典型柯伊伯纪暗色火成碎屑沉积物[10]（a~d）一未命名撞击坑（4.7°N，155.8°E）内的暗色火成碎屑沉积物；（b）中央峰内的白晕凹陷（白色箭头所示）和小型火山口（黄色箭头所示）；（c）暗色火成碎屑沉积物具有微弱的600 nm波段吸收特征（即BD600为正值）；（d）暗色火成碎屑沉积物覆盖了柯伊伯纪撞击坑的明亮溅射纹；（e~h）另一处直径约17 km的撞击坑（24.9°S，145.0°E）内外分布的暗色火成碎屑沉积物；（f）暗色火成碎屑沉积物中可见三处火山口（黄色箭头所示）；（g）暗色火成碎屑沉积物不具有微弱的600 nm波段吸收特征（即BD600为负值）；（h）暗色火成碎屑沉积物覆盖了北东侧新鲜撞击坑的溅射纹"

图10

水星表面火成碎屑沉积物的分布[77]"

图11

坑间平原和平坦平原N(20)密度[3]"

图12

坑间平原的地层序列[3]"

图13

水星表面平坦平原的绝对模式年龄[8]（a）平坦平原中央经度?年龄分布图，圆圈直径等比例对应平坦平原的面积；（b）不同成因平坦平原的年龄分布柱状图"

图14

拉赫马尼诺夫盆地内平原(左)和拉蒂特拉迪盆地内平原(右)的绝对模式年龄[8]"

图15

水星表面疑似侵入体"

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[1]  王大勇 1 ** , 陆现彩 2 , 徐士进 2 , 胡文瑄 2 , 齐 天 1 .  沉积盆地内侵入岩席对富含有机质围岩热影响的热传输模型研究 *

[J]. 南京大学学报(自然科学版), 2011, 47(1): 45-50.
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